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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2506.20564 |
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| _version_ | 1866915531491115008 |
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| author | Turner, Daisy A. Eschen, Yoshi Nike Emilia Murgas, Felipe Mortier, Annelies Wilson, Thomas G Fernández, Jorge Fernández Gromek, Nicole Morello, Giuseppe Tabernero, Hugo M. Egger, Jo Ann Vissapragada, Shreyas Caballero, José A. Dreizler, Stefan Freckelton, Alix Violet Hatzes, Artie P. Lakeland, Ben Scott Nagel, Evangelos Naponiello, Luca Vanaverbeke, Siegfried Venner, Alexander Osorio, María Rosa Zapatero Amado, Pedro J. Béjar, Víctor J. S. Bonomo, Aldo Stefano Buchhave, Lars A. Cameron, Andrew Collier Carleo, Ilaria Chaturvedi, Priyanka Cloutier, Ryan Damasso, Mario Daspute, Mangesh Dholakia, Shishir Dufoer, Sjoerd Dumusque, Xavier Fiorenzano, Aldo Fabricio Martinez Ghedina, Adriano Harutyunyan, Avet Herrero, Enrique John, Ancy Anna Lillo-Box, Jorge Lodieu, Nicolas López-Morales, Mercedes Malavolta, Luca Mancini, Luigi Mantovan, Giacomo Montes, David Morales, Juan Carlos Nicholson, Belinda Orell-Miquel, Jaume Palethorpe, Larissa Palle, Enric Quirrenbach, Andreas Reffert, Sabine Reiners, Ansgar Ribas, Ignasi Rice, Ken Silva, André M. Sozzetti, Alessandro Stalport, Manu Tal-Or, Lev Trifonov, Trifon Udry, Stéphane Zechmeister, Mathias |
| author_facet | Turner, Daisy A. Eschen, Yoshi Nike Emilia Murgas, Felipe Mortier, Annelies Wilson, Thomas G Fernández, Jorge Fernández Gromek, Nicole Morello, Giuseppe Tabernero, Hugo M. Egger, Jo Ann Vissapragada, Shreyas Caballero, José A. Dreizler, Stefan Freckelton, Alix Violet Hatzes, Artie P. Lakeland, Ben Scott Nagel, Evangelos Naponiello, Luca Vanaverbeke, Siegfried Venner, Alexander Osorio, María Rosa Zapatero Amado, Pedro J. Béjar, Víctor J. S. Bonomo, Aldo Stefano Buchhave, Lars A. Cameron, Andrew Collier Carleo, Ilaria Chaturvedi, Priyanka Cloutier, Ryan Damasso, Mario Daspute, Mangesh Dholakia, Shishir Dufoer, Sjoerd Dumusque, Xavier Fiorenzano, Aldo Fabricio Martinez Ghedina, Adriano Harutyunyan, Avet Herrero, Enrique John, Ancy Anna Lillo-Box, Jorge Lodieu, Nicolas López-Morales, Mercedes Malavolta, Luca Mancini, Luigi Mantovan, Giacomo Montes, David Morales, Juan Carlos Nicholson, Belinda Orell-Miquel, Jaume Palethorpe, Larissa Palle, Enric Quirrenbach, Andreas Reffert, Sabine Reiners, Ansgar Ribas, Ignasi Rice, Ken Silva, André M. Sozzetti, Alessandro Stalport, Manu Tal-Or, Lev Trifonov, Trifon Udry, Stéphane Zechmeister, Mathias |
| contents | Small temperate planets are prime targets for exoplanet studies due to their possible similarities with the rocky planets in the Solar System. M dwarfs are promising hosts since the planetary signals are within our current detection capabilities. Gliese 12 b is a Venus-sized temperate planet orbiting a quiet M dwarf. We present here the first precise mass measurement of this small exoplanet. We performed a detailed analysis using HARPS-N, ESPRESSO, and CARMENES radial velocities, along with new and archival \tess, \cheops, and MuSCAT2/3 photometry data. From fitting the available data, we find that the planet has a radius of $R_\mathrm{p} = 0.93\pm0.06 \,\mathrm{R_\oplus}$ and a mass of $M_\mathrm{p} = 0.95^{+0.29}_{-0.30} \,\mathrm{M_\oplus}$ (a $3.2σ$ measurement of the semi-amplitude $K=0.67\pm0.21\,\mathrm{m\,s^{-1}}$), and is on an orbit with a period of $12.761418^{+0.000060}_{-0.000055}\,\mathrm{d}$. A variety of techniques were utilised to attenuate stellar activity signals. Gliese 12 b has an equilibrium temperature of $T_\mathrm{eq}=317 \pm 8\,\mathrm{K}$, assuming an albedo of zero, and a density consistent with that of Earth and Venus ($ρ_\mathrm{p}=6.4\pm2.4\,\mathrm{g\,cm^{-3}}$). We find that Gliese 12 b has a predominantly rocky interior and simulations indicate that it is unlikely to have retained any of its primordial gaseous envelope. The bulk properties of Gliese 12 b place it in an extremely sparsely populated region of both mass--radius and density--$T_\mathrm{eq}$ parameter space, making it a prime target for follow-up observations, including Lyman-$α$ studies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_20564 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The mass of the exo-Venus Gliese 12 b, as revealed by HARPS-N, ESPRESSO, and CARMENES Turner, Daisy A. Eschen, Yoshi Nike Emilia Murgas, Felipe Mortier, Annelies Wilson, Thomas G Fernández, Jorge Fernández Gromek, Nicole Morello, Giuseppe Tabernero, Hugo M. Egger, Jo Ann Vissapragada, Shreyas Caballero, José A. Dreizler, Stefan Freckelton, Alix Violet Hatzes, Artie P. Lakeland, Ben Scott Nagel, Evangelos Naponiello, Luca Vanaverbeke, Siegfried Venner, Alexander Osorio, María Rosa Zapatero Amado, Pedro J. Béjar, Víctor J. S. Bonomo, Aldo Stefano Buchhave, Lars A. Cameron, Andrew Collier Carleo, Ilaria Chaturvedi, Priyanka Cloutier, Ryan Damasso, Mario Daspute, Mangesh Dholakia, Shishir Dufoer, Sjoerd Dumusque, Xavier Fiorenzano, Aldo Fabricio Martinez Ghedina, Adriano Harutyunyan, Avet Herrero, Enrique John, Ancy Anna Lillo-Box, Jorge Lodieu, Nicolas López-Morales, Mercedes Malavolta, Luca Mancini, Luigi Mantovan, Giacomo Montes, David Morales, Juan Carlos Nicholson, Belinda Orell-Miquel, Jaume Palethorpe, Larissa Palle, Enric Quirrenbach, Andreas Reffert, Sabine Reiners, Ansgar Ribas, Ignasi Rice, Ken Silva, André M. Sozzetti, Alessandro Stalport, Manu Tal-Or, Lev Trifonov, Trifon Udry, Stéphane Zechmeister, Mathias Earth and Planetary Astrophysics Small temperate planets are prime targets for exoplanet studies due to their possible similarities with the rocky planets in the Solar System. M dwarfs are promising hosts since the planetary signals are within our current detection capabilities. Gliese 12 b is a Venus-sized temperate planet orbiting a quiet M dwarf. We present here the first precise mass measurement of this small exoplanet. We performed a detailed analysis using HARPS-N, ESPRESSO, and CARMENES radial velocities, along with new and archival \tess, \cheops, and MuSCAT2/3 photometry data. From fitting the available data, we find that the planet has a radius of $R_\mathrm{p} = 0.93\pm0.06 \,\mathrm{R_\oplus}$ and a mass of $M_\mathrm{p} = 0.95^{+0.29}_{-0.30} \,\mathrm{M_\oplus}$ (a $3.2σ$ measurement of the semi-amplitude $K=0.67\pm0.21\,\mathrm{m\,s^{-1}}$), and is on an orbit with a period of $12.761418^{+0.000060}_{-0.000055}\,\mathrm{d}$. A variety of techniques were utilised to attenuate stellar activity signals. Gliese 12 b has an equilibrium temperature of $T_\mathrm{eq}=317 \pm 8\,\mathrm{K}$, assuming an albedo of zero, and a density consistent with that of Earth and Venus ($ρ_\mathrm{p}=6.4\pm2.4\,\mathrm{g\,cm^{-3}}$). We find that Gliese 12 b has a predominantly rocky interior and simulations indicate that it is unlikely to have retained any of its primordial gaseous envelope. The bulk properties of Gliese 12 b place it in an extremely sparsely populated region of both mass--radius and density--$T_\mathrm{eq}$ parameter space, making it a prime target for follow-up observations, including Lyman-$α$ studies. |
| title | The mass of the exo-Venus Gliese 12 b, as revealed by HARPS-N, ESPRESSO, and CARMENES |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2506.20564 |